Al Mueller BNL RHIC Neutrinos The Era of
Al Mueller - BNL RHIC Neutrinos: The Era of Long Baselines Large Detectors Intense Beams Nicholas P. Samios Columbia University, NYC October 23, 2009
Pleasure to be back at Columbia Occasion of Al’s 70 th Birthday Long, special relationship between BNL & Columbia Phd MIT 1965 (BS. Iowa State ’ 61) BNL 1965 – 1971 Postdoc – Ass’t Physicist Exciting years in both Weak Interactions, ν’s, V-A Strong Interactions – SU(3) Al is part of the distinguished alumni group Gary Feinberg Mel Schwartz ’ 59 – ’ 58 G. C. Wick ’ 57 – ’ 64
Member of many advisory committees at BNL High Energy & Nuclear Physics (1)Program Advisory Committee 1988 – 1992 L. Truman Chair 1988 – 1991 M. Schwartz Chair 1991 – 1994 BSA – Science and Technology Board 1998 – 2006 RBRC Scientific Review Committee to Present Large { { Unique Time: RHIC – Construction Call for Proposals ~ 1990 Under Mel – 11 Proposals Rejected Subsequently 4 Approved STAR, PHENIX, BRAHMS, PHOBOS Small 1990 – 1999 1991 – 1992
RBRC Policy Committee - 1991 Ozaki, Bock, Samios, Schiffer, Baym, Darriulat, Schwartz, Kerman Ball, Sandweiss, Lee, Symons, Henley, Hayakawa, Willis, Feshbach
A few words concerning RHIC The preamble to the RHIC Conceptual Design Report of 1989 is especially Prophetic: I quote, “The essential motivation for colliding nuclei at ultrarelativistic energies is the production of matter at extreme conditions of temperature and density: extended volumes of hadronic matter with energy densities greater than 10 times that of the nuclear ground state should be realizable. There is little direct knowledge about what to expect under such conditions. They have not been detected anywhere in the natural universe, and are just beginning to be approached through experiments with ion beams in experiments at Brookhaven and CERN. Thus the proposed facility represents a venture into an almost completely unknown regime for the study of basic properties of matter. While this leap into the unknown is by itself compelling attraction for both experimenters and theorists, it is also true that very specific goals for discovery and exploration can be defined within the present understanding of Quantum Chromodynamics (QCD) – as developed from high energy collisions of elementary particles – and the low energy behavior of bulk nuclear matter. The parameters of the proposed machine complex will allow the experimenter to make contact with both regimes in the systematic study of new phenomenon” RHIC has indeed created a new state of hot dense matter however behaving more like a liquid than a gas, the s. QGP. I would say that this dream envisioned for RHIC has been fulfilled
RHIC photo here
Neutrino History • • • 1930 1956 1962 1970 -91 1991 2000’s Existence – Postulated by Pauli Discovered Two Neutrinos Solar deficiency Three Neutrinos Neutrino Oscillations and Mass Kamiokande Super Kamiokande Sudbury Kamland KEK Minos and Others
Neutrino Parameters Mass Differences Mixing Angles
To be determined Value of θ 13 Mass hierarchy – sign of CP violation Precision Measurement of Why? Comparison with Quark mixing parameters Matter-Antimatter asymmetry Leptogenisis – Baryogenesis Other Benefits Proton Decay Supernovae
How? Large Detectors Water Cereknov ≥ 300 Ktons. (50 Kton) Liquid Argon ≥ 50 Ktons (. 6 kton) Intense Proton Beam I ≥ 1 Mwatt (. 3 Mwatt) Long Baseline L ≥ 1, 000 km (750 km) Wide Band Neutrino Beam. 5 – 5 Ge. V Appearance exp’t νμ→νμ ; Disappearance exp’t νμ→νe f(Δm 2, θ’s, L/E, earth matter)
Water Cherenkov Detector 1 module fid: 100 k. T 300 k. T
Event rate Evt rate: 1 MW for 3 yrs • • • Event type 300 k. T, 120 Ge. V 0. 5 deg. 300 k. T, 60 Ge. V 0 deg. Numu CC no osc 161820 272693 Numu CC with osc 68220 124479 neutrino spectrum High precision sin² 2θ 23, ∆m² 31 Important (esp. θ 23 ~ 45 deg. ) with possibility of new physics. Either 120 Ge. V or 60 Ge. V beam can be used: two oscillation nodes. Measurement dominated by systematics (see hep/0407047) (~1%) yr~2 x 107 sec
WBLE to DUSEL(1300 km) 3 sig, 5 sig discovery regions. 60 10^20 POT for each nu and anu 300 k. T WCh Stat+syst th 13 0. 004 mass ordering CP violation 0. 008 0. 01 CP Fraction: Fraction of the CP phase (0 -2 pi) covered at a particular confidence level. Report the value of th 13 at the 50% CP fraction.
• Program should lead to measurement of 3 -generation parameters without ambiguities. • CP measurement is approximately independent of θ 13 if not background limited. Need large detector independent of θ 13 value. 300 k. T water Cherenkov detector @DUSEL Measurement of CP phase and Sin² 2θ 13 at several points. All ambiguities and mass hierarchy are resolved.
Proton Decay Early Experiments IMB, Kolar Gold Mine, Homestake, Soudan, Frejus Recent Experiments Kameokande, Superkameokande Theory: SU(5) Minimal SUSY GUT SU(5) SO(10) Exp. Limits 1029 -1030 yrs 1028 -1030 yrs 2 x 1035 yrs 1034 yrs 8. 2 x 1033 yrs >2. 8 x 1033 yrs Super. K 141 kton yrs Next Order of Magnitude Again Need very large detectors
Supernova Neutrinos SN 87 A IMB Kameokande 19 Events Core Collapse of Supernova Dynamics Fundamental Neutrino Properties, including θ 13 and mass hierarchy Galactic Supernovae ~ 1 in 30 years ~ 100, 000 events in 10 kpc Diffuse (Relic) Supernova Continuous flux Measure Neutrino Number Energy 0 – 40 Me. V Time seconds Need many Large Detectors
Conclusions New Era: Large Scale detectors Intense Beams Long distances 300 Kton Water Cerenkov; 50 Kton liquid argon 1 – 2 Mwatts 1300 Km Fermilab – Homestake First Proposed (2003) Very Long Baseline Neutrino Oscillation Experiment for Precise Measurement of mixing Parameters and CP Violating Effects M. Diwan, W. Marciano et. al. Phys. Rev. D 68, 12002 (2003) Grand opportunity: Greatly improve accuracy of atmospheric and solar neutrino parameters Resolve value of Theta 13, mass hierarchy and possibly observe CP violation Observe Supernova Possibly observe proton decay DOE, NSF, Fermilab actually pursing such a neutrino program
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